arxiv: 1902.05554 · v2 · submitted 2019-02-14 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.HE

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First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback

Dylan Nelson , Annalisa Pillepich , Volker Springel , Ruediger Pakmor , Rainer Weinberger , Shy Genel , Paul Torrey , Mark Vogelsberger

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Federico Marinacci Lars Hernquist

Authors on Pith no claims yet

Pith reviewed 2026-05-16 10:52 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.HE

keywords galactic outflowssupernova feedbackblack hole feedbackcosmological simulationgalaxy stellar massmass loading factoroutflow velocitygalaxy quenching

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The pith

In this high-resolution cosmological simulation, galactic outflow mass loading turns non-monotonic with stellar mass and rises rapidly above 10^10.5 solar masses due to central black hole feedback.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines galactic outflows in a large-volume, high-resolution cosmological simulation with about 100 parsec resolution. It finds that the outflow mass loading factor, which measures how much gas is ejected compared to stars formed, decreases with increasing galaxy stellar mass at lower masses but then increases sharply at higher masses. This turnaround is attributed to the growing influence of feedback from the central supermassive black hole. The simulation also shows that outflows are faster at higher redshifts for the same mass and can include cool, dense gas phases moving at thousands of kilometers per second. Simple rules for energy injection at small scales lead to complex emergent behaviors like collimated bipolar outflows at larger scales.

Core claim

The central claim is that the outflow mass loading is a non-monotonic function of galaxy stellar mass, turning over and rising rapidly above 10^10.5 solar masses due to the action of the central black hole. Outflow velocity increases with stellar mass, and at fixed mass is faster at higher redshift. The model produces high velocity, multi-phase outflows including cool, dense components that reach speeds in excess of 3000 km/s. Despite isotropic wind launching, outflows exhibit natural collimation and an emergent bipolarity. Galaxies above the star-forming main sequence drive faster outflows, although this correlation inverts at high mass with the onset of quenching driven by low-luminosity,

What carries the argument

Subgrid feedback prescriptions for supernovae and black holes that drive winds and inject energy at the simulation's resolution scale.

If this is right

Outflow mass loading decreases then rises with galaxy stellar mass.
Outflow speeds increase with galaxy mass and are higher at earlier times.
Outflows develop collimated bipolar structures from isotropic launching.
Stronger outflows occur in galaxies above the star formation main sequence, inverting at high masses during quenching.
Multi-phase outflows with high-velocity cool components are generated.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

Black hole feedback may be responsible for quenching star formation in massive galaxies by driving strong outflows.
The predicted mass dependence of outflows could be tested with current and future astronomical observations of gas kinematics.
The results highlight how small-scale feedback processes influence large-scale galaxy evolution in complex ways.
Similar simulations at even higher resolution could check if these outflow properties remain stable.

Load-bearing premise

The subgrid prescriptions for supernova and black hole feedback are assumed to produce realistic large-scale outflows at the simulation's median resolution of about 100 parsecs.

What would settle it

Direct measurements of outflow mass loading in galaxies more massive than 10^10.5 solar masses showing no increase or a continued decrease would falsify the non-monotonic behavior driven by black hole feedback.

read the original abstract

We present the new TNG50 cosmological, magnetohydrodynamical simulation -- the third and final volume of the IllustrisTNG project. This simulation occupies a unique combination of large volume and high resolution, with a 50 Mpc box sampled by 2160^3 gas cells (baryon mass of 8x10^4 Msun). The median spatial resolution of star-forming ISM gas is ~100-140 parsecs. This resolution approaches or exceeds that of modern 'zoom' simulations of individual massive galaxies, while the volume contains ~20,000 resolved galaxies with M*>10^7 Msun. Herein we show first results from TNG50, focusing on galactic outflows driven by supernovae as well as supermassive black hole feedback. We find that the outflow mass loading is a non-monotonic function of galaxy stellar mass, turning over and rising rapidly above 10^10.5 Msun due to the action of the central black hole. Outflow velocity increases with stellar mass, and at fixed mass is faster at higher redshift. The TNG model can produce high velocity, multi-phase outflows which include cool, dense components. These outflows reach speeds in excess of 3000 km/s out to 20 kpc with an ejective, BH-driven origin. Critically, we show how the relative simplicity of model inputs (and scalings) at the injection scale produces complex behavior at galactic and halo scales. For example, despite isotropic wind launching, outflows exhibit natural collimation and an emergent bipolarity. Furthermore, galaxies above the star-forming main sequence drive faster outflows, although this correlation inverts at high mass with the onset of quenching, whereby low luminosity, slowly accreting, massive black holes drive the strongest outflows.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

TNG50 supplies a new statistical sample of outflows at 100 pc resolution across 20k galaxies, with clear emergent trends, though the specific tie of the high-mass mass-loading upturn to black hole feedback rests on the tuned model without an isolating control.

read the letter

TNG50 combines a 50 Mpc volume with roughly 100 pc resolution for the star-forming gas, which is the new element here. That setup yields about 20,000 galaxies above 10^7 solar masses, enough to measure outflow mass loading, velocity, and phase structure as functions of stellar mass and redshift in a single run. The paper reports that mass loading falls with mass up to around 10^10.5 solar masses then rises sharply, that outflow speeds increase with mass and are higher at earlier times, and that the winds show natural collimation into bipolar patterns even though the injection is isotropic. It also notes that galaxies above the star-forming sequence drive faster outflows until quenching sets in at high mass, where slowly accreting black holes take over. These are direct measurements from the snapshots rather than analytic derivations, and the work shows how the relatively simple subgrid scalings produce multi-phase, high-velocity flows that reach beyond 20 kpc. The scale and the emergent behavior are the parts that hold up cleanly. The simulation volume and resolution are genuinely new for the TNG series, and the statistics let them bin trends without the small-number problems that plague zoom runs. The collimation and the reversal of the star-formation-rate correlation at high mass are useful outputs that follow from the model without extra tuning. The soft spot is the causal claim on the mass-loading upturn. The abstract and first-results section attribute the rise above 10^10.5 solar masses to central black hole action, but the text does not describe a no-black-hole control run or a decomposition that subtracts the supernova-driven component at fixed mass and resolution. At the stated resolution, numerical coupling between the two feedback channels could contribute, so the specific assignment remains tied to the full tuned model rather than isolated. The feedback efficiencies themselves were set in earlier TNG papers, which is normal practice but limits how independently the result tests the physics. This is for groups that run or compare against large-volume galaxy formation simulations and need outflow benchmarks at this resolution. It deserves a serious referee because the dataset is substantial and the reported trends are internally consistent with the simulation outputs. A reviewer could reasonably ask for the control comparison or more detail on outflow identification, but the core results are worth that step rather than a desk reject.

Referee Report

1 major / 1 minor

Summary. The manuscript presents first results from the TNG50 cosmological magnetohydrodynamical simulation (50 Mpc box, 2160^3 gas cells, baryon mass resolution 8e4 Msun, median ISM resolution ~100-140 pc). Focusing on galactic outflows, it reports that the outflow mass-loading factor is a non-monotonic function of galaxy stellar mass, turning over and rising rapidly above 10^10.5 Msun due to central black hole feedback. Additional findings include increasing outflow velocity with stellar mass and redshift, production of high-velocity (>3000 km/s) multi-phase outflows with ejective BH-driven components, natural collimation and bipolarity despite isotropic injection, and an inversion of the star-forming main-sequence correlation at high mass due to quenching.

Significance. If the trends are robust, the work provides a statistically significant view of feedback-driven outflows across ~20,000 resolved galaxies, illustrating how simple subgrid prescriptions for supernova winds and black hole feedback can yield complex emergent behavior at galactic scales. The combination of large volume and high resolution allows direct comparison to observations of multi-phase outflows and has implications for the role of AGN feedback in quenching massive galaxies.

major comments (1)

[Abstract] Abstract: The central claim that the mass-loading upturn above 10^{10.5} Msun arises specifically from central black hole action is not supported by any referenced control simulation without BH feedback or by a decomposition that isolates the BH-driven component at fixed resolution and galaxy mass. Without such a test, the causal attribution remains unverified given the ~100 pc resolution and the calibrated subgrid wind scalings.

minor comments (1)

The abstract refers to 'the TNG model' without restating the key supernova wind velocity/mass-loading scalings or black hole feedback efficiency parameters; a short recap would improve accessibility for readers not familiar with prior TNG papers.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and for recognizing the statistical power and scientific implications of the TNG50 results. We address the single major comment below and have made a targeted revision to improve the clarity of our causal attribution.

read point-by-point responses

Referee: [Abstract] Abstract: The central claim that the mass-loading upturn above 10^{10.5} Msun arises specifically from central black hole action is not supported by any referenced control simulation without BH feedback or by a decomposition that isolates the BH-driven component at fixed resolution and galaxy mass. Without such a test, the causal attribution remains unverified given the ~100 pc resolution and the calibrated subgrid wind scalings.

Authors: We agree that a dedicated control run without black hole feedback at TNG50 resolution and volume would constitute the most direct test. No such simulation exists in our current suite. Our attribution instead rests on the internal structure of the TNG model: the supernova wind mass-loading scaling is explicitly mass-independent at injection and produces a declining trend with stellar mass when BH feedback is absent (as demonstrated in the lower-resolution TNG100 and TNG300 runs and in the original model calibration papers). The upturn appears only once the BH feedback channel is active, and the high-mass outflow properties (velocity, temperature, and multi-phase structure) match the expectations of the BH-driven wind implementation. To address the referee’s concern we have revised the abstract to replace “due to the action of the central black hole” with “associated with the onset of efficient black hole feedback” and have added a short clarifying paragraph in Section 3.2 that references the model behavior in the absence of BHs. revision: partial

Circularity Check

0 steps flagged

No significant circularity: reported trends are direct simulation measurements

full rationale

The paper reports emergent galactic outflow properties measured directly from TNG50 simulation snapshots at ~100 pc resolution. The non-monotonic mass-loading trend with stellar mass is presented as a simulation outcome, not an algebraic derivation or fitted parameter. Subgrid feedback prescriptions originate in prior TNG work, but the current claims do not reduce to those inputs by construction, nor invoke self-citations as load-bearing uniqueness theorems. No self-definitional, fitted-prediction, or ansatz-smuggling steps appear in the abstract or described results. The work is self-contained as a first-results report of simulation outputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on subgrid feedback models whose parameters were calibrated in prior TNG work; the simulation itself solves standard hydrodynamics and gravity on the supplied grid.

free parameters (2)

supernova wind velocity and mass loading scalings
Tuned in the TNG model to reproduce the stellar mass function and other observables; directly control the low-mass outflow behavior.
black hole feedback efficiency and coupling
Calibrated to quench massive galaxies; responsible for the reported upturn above 10^10.5 Msun.

axioms (2)

standard math Standard Lambda-CDM cosmology and initial conditions from Planck parameters
Invoked to set the background expansion and initial density field.
domain assumption Subgrid ISM pressurization and star formation threshold
Assumed to produce realistic star-forming gas at the ~100 pc resolution.

pith-pipeline@v0.9.0 · 5674 in / 1504 out tokens · 33212 ms · 2026-05-16T10:52:37.934537+00:00 · methodology

discussion (0)

Forward citations

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